Note: although all panel members are members of the LIGO Scientific Collaboration, the opinions expressed here are not necessarily those of the LSC. When possible, we link documents and policies by the LSC.
Open questions that the LSC is discussing. No conclusions, yet, so this is only a guide and not a definitive statement of the collaboration.(Duncan, Gaby)
We'll likely have several runs with of increasing duration and sensitivity, probably starting in 2015.
When does it make sense to have a first short science run? Perhaps some time in 2015+ we will have BNS range of 50 - 100 Mpc. Run of a couple of months?
When should we have first extended science runs? Sometime in 2016+ we will have BNS ranges 100 - 140 Mpc. Run of order six months?
When will we all the aLIGO detectors be at design sensitivity? Full zero-detune high-power will follow, and will take years. Guess for when this will be? 2018-19+ with BNS sensitivity 140-200 Mpc?
Virgo will be part of these as soon as available.
KAGRA plans to have a non-cryogenic detector with sensitivity similar to initial LIGO detectors by 2015, and reach increased sensitivity with cryogenic by 2018.
Noise curves for early aLIGO runs: tentative and subject to caveats above!(Duncan)
(Samaya) early years of Ligo Hanford and Livingston: possibly >three incremental runs until design sensitivity is reached. A tentative starting date is @ the end of December 2014.
i) lower laser power and no signal recycling
ii) lower laser power and signal recycling
iii) full laser power and signal recycling
Noise curves should be shown and the improvement in sensitivity should be indicated at different frequency runs. Discussion of possible GW+EM science in the period 2015-17 using only two LIGO detectors (with no Virgo) is important.
(Samaya): Virgo: one year delay of advanced LIGO -- 2017-2018+ for three detectors.
(Samaya): Discussion of calibration.
Beyond aLIGO/AdVirgo: Upgrades to existing facilities
(Samaya) Discussion of optical squeezing and at what stage it will be implemented, and possible gains.
(Duncan, Gaby): currently instrumental teams are scoping out possible upgrades within the LIGO facilities. Some details in 2011 LSC instrumental white paper, more details will appear in 2012 white paper later this year.
Third-generation detectors.
(Samaya). A mention of tentative plans for the follow-on to advanced LIGO.
(Duncan, Gaby) Europeans have an Einstein Telecope design document available from http://www.et-gw.eu/
(Duncan, Gaby) No major funded US effort right now, focus is on R&D components.
What's the status of LIGO-India?
(Gaby) The LIGO Lab has recommended NSF to approve LIGO-India; NSF and NSB are seriously considering this recommendation.
If approved and everything goes well, a LIGO-India detector could join the Advanced Detectors network by ~2020 - see below.
(Samaya). What are the main challenges for LIGO India in terms of instrument construction?
(Gaby) The instrument itself would be the LIGO H2 detector, so there shouldn't be any challenges that are not seen first with L1 and H1. The challenges are instead on the Observatory construction (including site selection and vacuum system), and commissioning. Commissioning should be helped by earlier experience with L1 and H1, but it's always a challenge.
Comparison of aLIGO USA and LIGO-India timelines (Duncan, (thanks to David Shoemaker)). Subject to NSF and NSB approval!
If we get approval, this is how we would proceed.
aLIGO-USA
Planned LIGO-India
Oct 2011: Installation start
May 2012: Integrated test start
Jul 2012: corner Michelson testing
Mid 2012: Project start
July 2013: All installation complete
Mid 2013: Contractors selected
Nov 2014: All interferometers accepted
Mid 2014: Start site development
2015: Possible first observing run
2015:Construction well underway
2017: Higher sensitivity runs
2017: Ship instrument to India
2018: Facility ready, start install
2019: installation complete
Early 2020: interferometer accepted
Mid 2020: First science run
(Samaya). How does LIGO-India help in sky reconstruction? (see Veitch et al. (2012) and Schutz (2011))
What are the goals for science analysis in the Advanced detector era?
These can be found in the 2011 Data Analysis white paper. We'll perform searches we've done in S5/S6 (unmodeled transient sources, binary systems, rotating stars and stochastic background), but with more of the searches for transients using a low latency, sky localization and conservative but reliable and fast false alarm estimate to be able to produce alerts to EM/HE partners.
With what latency and accuracy can positional and intrinsic information be provided, eg for EM followup? (Richard)
(Samaya). Discussion of LSC parameter estimation group and low latency group pipelines. Latency of 45 mins (human limited) is S6 for initial sky reconstruction maps.
Advanced LIGO: latency of ~10 minutes (?).
Sky localization--be prepared for 1-100 (or 100s sq. deg for the first couple of years with Virgo running) sq. deg accuracies depending on whether the signal is threshold/: plethora of papers in recent years for burst/inspirals in advanced LIGO- Wen and Chen (2010), Fairhurst (2009,2010), Klimenko et al. (2010), Nissanke et al (2011), Veitch et al. (2012)
PCTS Workshop Day 1 Talks:
Patrick Brady
Peter Shawhan
PCTS Workshop Day 1 Discussion Panel:
Note: although all panel members are members of the LIGO Scientific Collaboration, the opinions expressed here are not necessarily those of the LSC. When possible, we link documents and policies by the LSC.
Questions:
(Samaya) early years of Ligo Hanford and Livingston: possibly >three incremental runs until design sensitivity is reached. A tentative starting date is @ the end of December 2014.
i) lower laser power and no signal recycling
ii) lower laser power and signal recycling
iii) full laser power and signal recycling
Noise curves should be shown and the improvement in sensitivity should be indicated at different frequency runs. Discussion of possible GW+EM science in the period 2015-17 using only two LIGO detectors (with no Virgo) is important.
(Samaya): Virgo: one year delay of advanced LIGO -- 2017-2018+ for three detectors.
(Samaya): Discussion of calibration.
(Samaya) Discussion of optical squeezing and at what stage it will be implemented, and possible gains.
(Duncan, Gaby): currently instrumental teams are scoping out possible upgrades within the LIGO facilities. Some details in 2011 LSC instrumental white paper, more details will appear in 2012 white paper later this year.
(Samaya). A mention of tentative plans for the follow-on to advanced LIGO.
(Duncan, Gaby) Europeans have an Einstein Telecope design document available from http://www.et-gw.eu/
(Duncan, Gaby) No major funded US effort right now, focus is on R&D components.
(Gaby) The LIGO Lab has recommended NSF to approve LIGO-India; NSF and NSB are seriously considering this recommendation.
If approved and everything goes well, a LIGO-India detector could join the Advanced Detectors network by ~2020 - see below.
(Samaya). What are the main challenges for LIGO India in terms of instrument construction?
(Gaby) The instrument itself would be the LIGO H2 detector, so there shouldn't be any challenges that are not seen first with L1 and H1. The challenges are instead on the Observatory construction (including site selection and vacuum system), and commissioning. Commissioning should be helped by earlier experience with L1 and H1, but it's always a challenge.
Comparison of aLIGO USA and LIGO-India timelines (Duncan, (thanks to David Shoemaker)). Subject to NSF and NSB approval!
If we get approval, this is how we would proceed.
(Samaya). How does LIGO-India help in sky reconstruction? (see Veitch et al. (2012) and Schutz (2011))
These can be found in the 2011 Data Analysis white paper. We'll perform searches we've done in S5/S6 (unmodeled transient sources, binary systems, rotating stars and stochastic background), but with more of the searches for transients using a low latency, sky localization and conservative but reliable and fast false alarm estimate to be able to produce alerts to EM/HE partners.
(Samaya). Discussion of LSC parameter estimation group and low latency group pipelines. Latency of 45 mins (human limited) is S6 for initial sky reconstruction maps.
Advanced LIGO: latency of ~10 minutes (?).
Sky localization--be prepared for 1-100 (or 100s sq. deg for the first couple of years with Virgo running) sq. deg accuracies depending on whether the signal is threshold/: plethora of papers in recent years for burst/inspirals in advanced LIGO- Wen and Chen (2010), Fairhurst (2009,2010), Klimenko et al. (2010), Nissanke et al (2011), Veitch et al. (2012)
Toward Early-Warning Detection of Gravitational Waves from Compact Binary Coalescence
(Gaby) LSC and Virgo are finalizing the approval of a policy shown here:
(Gaby) The official LIGO/LSC policy for open data is found here.
(Gaby) LSC and Virgo are having conversations with KAGRA about a data-sharing agreement.
(Samaya). Public LIGO open data documents
http://www.ligo.caltech.edu/gwodw2011/program.shtml
https://dcc.ligo.org/public/0076/P1100182/001/ReportGWODW2.pdf
(Samaya). some mention of Virgo/KAGRA etc's plans would be useful.